SHOCK FRONTS ARE HYDRODYNAMICAL DISCONTINUITIES THAT PROPAGATE AT SUPERSONIC SPEEDS. ON COSMOLOGICAL SCALES THEY PLAY A KEY ROLE IN HIERARCHICAL STRUCTURE FORMATION: AS GAS STREAMS ALONG INTERGALACTIC FILAMENTS IT IS SLOWED DOWN AND HEATED UP AT STRONG ACCRETION SHOCKS ON THE OUTSKIRTS OF GALAXY AND CLUSTER HALOS. GALAXY MERGERS ALSO DRIVE MODERATE-STRENGTH SHOCK WAVES INTO THE INTRACLUSTER MEDIUM. ON SMALLER SCALES ACTIVE GALACTIC NUCLEI (AGN) GENERATE SHOCKS THAT CONVERT KINETIC ENERGY INTO THERMAL ENERGY COMPLETING A BLACK HOLE (BH) FEEDBACK LOOP THAT IS ESSENTIAL FOR GALAXY EVOLUTION. THANKS TO RECENT ADVANCES SUCH AS THE ADDITION OF MAGNETIC FIELDS AND LARGER SIMULATED VOLUMES COSMOLOGICAL SIMULATIONS CAN NOW CAPTURE THE WIDE DIVERSITY OF SHOCK STRENGTHS AND MORPHOLOGIES FOUND IN OUR UNIVERSE. THE GOAL OF THIS PROPOSAL IS TO STUDY SHOCKS IN THE ILLUSTRISTNG COSMOLOGICAL SIMULATIONS WHICH MODEL THE EVOLUTION OF GAS DARK MATTER MAGNETIC FIELDS AS WELL AS STARS AND BHS TOGETHER WITH THEIR ASSOCIATED FEEDBACK PROCESSES. USING THE OUTPUT OF A SHOCK FINDER ALGORITHM THAT WAS RUN ON-THE-FLY IN ILLUSTRISTNG WE WILL STUDY THE DISTRIBUTIONS OF THE TOTAL SHOCK SURFACE AREA THE ENERGY DISSIPATION RATE AND THE RANGE OF SHOCK MACH NUMBERS OVER A LARGE COSMOLOGICAL BOX. THE FIRST OBJECTIVE OF OUR PROJECT IS TO TEST HOW SHOCK PROPERTIES DEPEND ON THE BLACK HOLE FEEDBACK PRESCRIPTION. WE WILL PROVIDE PREDICTIONS FOR INTEGRAL FIELD OBSERVATIONS OF SHOCKS PRODUCED BY THE NEW KINETIC AGN FEEDBACK MODE IN ILLUSTRISTNG AND COMPARE TO CURRENT OBSERVATIONS OF FR 0 AND RED GEYSER GALAXIES. THESE OBSERVATIONAL CONSTRAINTS ARE CRUCIAL FOR DEVELOPING FUTURE MODELS OF AGN FEEDBACK IN COSMOLOGICAL SIMULATIONS